Solar coronal loops and coronal heating models

Ever since it was realized, some sixty five years ago, that the solar corona is three orders of magnitude hotter than the underlying photosphere, scientists have puzzled over the reason for these extreme conditions. A number of plausible ideas have been put forward, including the dissipation of magn...

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Detalles Bibliográficos
Publicado: 2005
Materias:
Corona
Coronal loops
Electric and magnetic fields
Holes
Streamers
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v784_n_p103_Mandrini
http://hdl.handle.net/20.500.12110/paper_0094243X_v784_n_p103_Mandrini
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0094243X_v784_n_p103_Mandrini
record_format dspace
spelling paper:paper_0094243X_v784_n_p103_Mandrini2023-06-08T15:09:15Z Solar coronal loops and coronal heating models Corona Coronal loops Electric and magnetic fields Holes Streamers Ever since it was realized, some sixty five years ago, that the solar corona is three orders of magnitude hotter than the underlying photosphere, scientists have puzzled over the reason for these extreme conditions. A number of plausible ideas have been put forward, including the dissipation of magnetohydrodynamic (MHD) waves and the dissipation of stressed, current-carrying magnetic fields. Unfortunately, the conversion of magnetic to thermal energy occurs on spatial scales that are far smaller than can be observed directly by present-day solar instruments, and it has been extremely difficult to identify the exact cause of the heating. We will describe two different approaches we have undertaken combining soft X-ray coronal observations and photospheric magnetic observations with other indirect means (e.g. magnetic field extrapolations, quasi-static loop theory), to discriminate between the models that have been so far proposed to explain the coronal heating problem. Both approaches show that models based on the dissipation of stressed, current-carrying magnetic fields are in better agreement with the observations than models that attribute coronal heating to the dissipation of MHD waves injected at the base of the corona. © 2005 American Institute of Physics. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v784_n_p103_Mandrini http://hdl.handle.net/20.500.12110/paper_0094243X_v784_n_p103_Mandrini
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Corona
Coronal loops
Electric and magnetic fields
Holes
Streamers
spellingShingle Corona
Coronal loops
Electric and magnetic fields
Holes
Streamers
Solar coronal loops and coronal heating models
topic_facet Corona
Coronal loops
Electric and magnetic fields
Holes
Streamers
description Ever since it was realized, some sixty five years ago, that the solar corona is three orders of magnitude hotter than the underlying photosphere, scientists have puzzled over the reason for these extreme conditions. A number of plausible ideas have been put forward, including the dissipation of magnetohydrodynamic (MHD) waves and the dissipation of stressed, current-carrying magnetic fields. Unfortunately, the conversion of magnetic to thermal energy occurs on spatial scales that are far smaller than can be observed directly by present-day solar instruments, and it has been extremely difficult to identify the exact cause of the heating. We will describe two different approaches we have undertaken combining soft X-ray coronal observations and photospheric magnetic observations with other indirect means (e.g. magnetic field extrapolations, quasi-static loop theory), to discriminate between the models that have been so far proposed to explain the coronal heating problem. Both approaches show that models based on the dissipation of stressed, current-carrying magnetic fields are in better agreement with the observations than models that attribute coronal heating to the dissipation of MHD waves injected at the base of the corona. © 2005 American Institute of Physics.
title Solar coronal loops and coronal heating models
title_short Solar coronal loops and coronal heating models
title_full Solar coronal loops and coronal heating models
title_fullStr Solar coronal loops and coronal heating models
title_full_unstemmed Solar coronal loops and coronal heating models
title_sort solar coronal loops and coronal heating models
publishDate 2005
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v784_n_p103_Mandrini
http://hdl.handle.net/20.500.12110/paper_0094243X_v784_n_p103_Mandrini
_version_ 1768544678726074368

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